揭示磁层顶边界层中太阳风与行星离子的混合与传输过程
Unveiling the Mixing and Transport Processes of Solar Wind and Planetary Ions in the Magnetopause Boundary Layer
AI总结：
本研究采用三维全局混合模拟，从动力学视角定量揭示了太阳风条件如何通过 Kelvin-Helmholtz 波控制太阳风进入地球磁层顶及其与磁层离子的混合过程。
摘要：
Kelvin-Helmholtz (KH) 涡旋在天体物理学和日层物理学中被广泛观测到，包括木星和地球磁层顶、火星鞘层-电离层边界、日层顶以及恒星吸积盘内部。这些涡旋在跨边界层传输质量、动量和能量方面发挥着关键作用。与地球等有磁场行星相比，火星等无磁场行星表现出更高的完全卷起非线性 KH 涡旋发生率。与以往的磁流体力学 (MHD) 研究不同，本研究采用动力学视角，利用三维全局混合模拟（以地球为代表性案例）来量化离子混合率。该方法能够自动识别由 KH 调制的波纹状磁层顶。我们首次定量评估了太阳风条件如何通过 KH 波控制太阳风的进入及其随后与磁层离子的混合。我们发现，在北向行星际磁场 (IMF) 条件下，穿过日侧磁层顶的粒子通量随太阳风动压增加而增加，并在 KH 区域达到峰值。值得注意的是，由 KH 调制的低纬边界层随着动压增加而变薄。在南向 IMF 条件下，耦合的重联和 KH 结构进一步增强了太阳风的注入，并促进了日侧磁层离子的逃逸，特别是在重联加剧这种交换的日下点附近。这些结果也为日层及更远区域中有磁场行星的空间环境演化与质量传输提供了新见解。
英文摘要：
Kelvin-Helmholtz (KH) vortices are widely observed in astrophysics and heliophysics, including at Jovian and terrestrial magnetopauses, the Martian sheath-ionosphere boundary, the heliopause, and within stellar accretion disks. These vortices play a critical role in transporting mass, momentum, and energy across boundary layers. Magnetized planets such as Earth exhibit a higher incidence of fully rolled-up, nonlinear KH vortices compared to non-magnetized planets like Mars. In contrast to previous magnetohydrodynamic (MHD) studies, this work adopts a kinetic point of view to quantify ion mixing rates using three-dimensional global hybrid simulations, with Earth as a representative case. This approach enables automated identification of the KH-modulated, corrugated magnetopause. For the first time, we provide a quantitative assessment of how solar wind conditions control solar wind entry and subsequent mixing with magnetospheric ions via KH waves. We find that under northward interplanetary magnetic field (IMF) conditions, the flux of particles crossing the dayside magnetopause increases with solar wind dynamic pressure and peaks in the KH region. Notably, the KH-modulated low-latitude boundary layer thins as the dynamic pressure increases. Under southward IMF conditions, coupled reconnection and KH structures further enhance solar wind injection and boost magnetospheric ion escape in the dayside, especially near the subsolar point where reconnection intensifies this exchange. These results also shed light on the evolution of space environments and mass transport at magnetized planets in the heliosphere and beyond.
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